A protocluster at z = 2.45
- Institute for Astronomy, Department of Physics, ETH Zurich, Zurich 8093 (Switzerland)
- European Southern Observatory, Alonso de Córdova 3107, Casilla 19001, Vitacura, Santiago (Chile)
- INAF, Osservatorio Astronomico di Bologna, Via Ranzani 1, I-40127, Bologna (Italy)
- Instituto de Astrofísica, Facultad de Física, Pontificia Universidad Católica de Chile, Av. Vicuña Mackenna 4860, 782–0436 Macul, Santiago (Chile)
- Spitzer Science Center, 314–6 Caltech, Pasadena, CA 91125 (United States)
- Aix Marseille Université, CNRS, LAM (Laboratoire d’Astrophysique de Marseille) UMR 7326, F-13388, Marseille (France)
We present the spectroscopic confirmation of a z = 2.45 protocluster. Its member galaxies lie within a radius of 1.4 Mpc (physical) on the sky and within Δv±700 km s{sup −1} along the line of sight. We estimate an overdensity of 10, suggesting that the structure has made the turnaround but is not assembled yet. A comparison to the Millennium simulation suggests that analogous structures evolve into 10{sup 14}–10{sup 15} M{sub ⊙} h{sup −1} type dark matter halos by z = 0, qualifying the notion of “protocluster.” The search for the complete census of mock progenitor galaxies at z∼2.5 of these massive z = 0 mock clusters reveals that they are widely spread over areas with a diameter of 3–20 Mpc. This suggests that the optical selection of such protoclusters can result in a rich diversity regarding their z = 0 descendants. We also searched for signs of environmental differentiation in this protocluster. While we see a weak trend for more massive and more quiescent galaxies within the protocluster, this is not statistically significant.
- OSTI ID:
- 22883305
- Journal Information:
- Astrophysical Journal, Journal Name: Astrophysical Journal Journal Issue: 1 Vol. 802; ISSN ASJOAB; ISSN 0004-637X
- Country of Publication:
- United Kingdom
- Language:
- English
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